Notes:
- 1) The fitting includes the systematic errors.
- 2) When the burst includes telescope slew time periods, the fitting uses an average response file made from multiple 5-s response files through out the slew time plus single time preiod for the non-slew times, and weighted by the total counts in the corresponding time period using addrmf. An average response file is needed becuase a spectral fit using the pre-slew DRM will introduce some errors in both a spectral shape and a normalization if the PHA file contains a lot of the slew/post-slew time interval.
- 3) For fits to more complicated models (e.g. a power-law over a cutoff power-law), the BAT team has decided to require a chi-square improvement of more than 6 for each extra dof.
Time averaged spectrum fit using the average DRM
Power-law model
Time interval is from -0.032 sec. to 0.608 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.03003 ( -0.394991 0.421338 )
Norm@50keV : 8.78548E-03 ( -0.00203013 0.0019696 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 45.56 using 59 PHA bins.
# Reduced chi-squared = 0.7992 for 57 degrees of freedom
# Null hypothesis probability = 8.620880e-01
Photon flux (15-150 keV) in 0.64 sec: 1.01326 ( -0.237527 0.23897 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.01727e-08 ( -1.36291e-08 1.36143e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.032 sec. to 0.608 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.02316 ( -0.399346 0.467607 )
Epeak [keV] : 9999.31 ( -9999.36 -9999.36 )
Norm@50keV : 8.83465E-03 ( -0.00198791 0.0132005 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 45.56 using 59 PHA bins.
# Reduced chi-squared = 0.8137 for 56 degrees of freedom
# Null hypothesis probability = 8.391205e-01
Photon flux (15-150 keV) in 0.64 sec: 1.01307 ( -0.23761 0.2389 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.00454e-08 ( -1.72024e-08 1.74489e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.212 sec. to 0.788 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.960109 ( -0.487181 0.54844 )
Norm@50keV : 5.31465E-03 ( -0.0015915 0.00152664 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.48 using 59 PHA bins.
# Reduced chi-squared = 0.8330 for 57 degrees of freedom
# Null hypothesis probability = 8.114182e-01
Photon flux (15-150 keV) in 1 sec: 0.610796 ( -0.179685 0.182401 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.83109e-08 ( -1.65961e-08 1.66923e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.212 sec. to 0.788 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.12809 ( -1.96888 3.20137 )
Epeak [keV] : 42.8343 ( )
Norm@50keV : 3.67527E-04 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.15 using 59 PHA bins.
# Reduced chi-squared = 0.8420 for 56 degrees of freedom
# Null hypothesis probability = 7.940734e-01
Photon flux (15-150 keV) in 1 sec: 0.607528 ( -0.184449 0.177595 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.81661e-08 ( -1.6828e-08 1.67508e-08 ) ergs/cm2
Time-resolved spectra
